The remarkable properties of the symbiotic star AE Circinus

Mennickent, R. E.; Greiner, J.; Arenas, J.; Tovmassian, G.; Mason, E.; Tappert, C.; Papadaki, C.

doi:10.1111/j.1365-2966.2007.12604.x

Cited by 5 publications

(5 citation statements)

References 38 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…However, those objects also exhibit the 6545 Å line, which usually is attributed to the Raman scattered He ii line that is not detected in our data. Both the 6578 Å and 6581 Å lines have also been detected in the symbiotic star AE Circinus, and identified as carbon lines (Mennickent et al 2008). The 5002 Å line has been detected in the J320 (PNG190.317.7) nebula but no identification was provided (Harman et al 2004).…”

Section: Kinematicsmentioning

confidence: 99%

Evidence for a [WR] or WEL-type binary nucleus in the bipolar planetary nebula Vy 1-2

Akras

Boumis

Meaburn

et al. 2015

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

We present high-dispersion spectroscopic data of the compact planetary nebula Vy 1-2, where high expansion velocities up to 100 km s −1 are found in the Hα, [N ii] and [O iii] emission lines. HST images reveal a bipolar structure. Vy 1-2 displays a bright ring-like structure with a size of 2.4 ′′ ×3.2 ′′ and two faint bipolar lobes in the west-east direction. A faint pair of knots is also found, located almost symmetrically on opposite sides of the nebula at PA=305 • . Furthermore, deep low-dispersion spectra are also presented and several emission lines are detected for the first time in this nebula, such as the doublet [Cl iii] 5517, 5537Å, [K iv] 6101Å, C ii 6461Å, the doublet C iv 5801, 5812Å. By comparison with the solar abundances, we find enhanced N, depleted C and solar O. The central star must have experienced the hot bottom burning (CNcycle) during the 2 nd dredge-up phase, implying a progenitor star of M 3 M ⊙ . The very low C/O and N/O abundance ratios suggest a likely post-common envelope close binary system.A simple spherically symmetric geometry with either a blackbody or a H-deficient stellar atmosphere model is not able to reproduce the ionisation structure of Vy 1-2. The effective temperature and luminosity of its central star indicate a young nebula located at a distance of ∼9.7 kpc with an age of ∼3500 years. The detection of stellar emission lines, C ii 6461Å, the doublet C ivλλ 5801, 5812 and O iii 5592Å, emitted from a H-deficient star, indicates the presence of a late-type Wolf-Rayet or a WEL type central star.

show abstract

Section: Kinematicsmentioning

confidence: 99%

Evidence for a [WR] or WEL-type binary nucleus in the bipolar planetary nebula Vy 1-2

Akras

Boumis

Meaburn

et al. 2015

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

show abstract

“…This would explain its absence in our VLT FLAMES spectroscopy. Dusty cocoons appear in the symbiotic stars RX Pup (Mikołajewska et al 1999), other symbiotic Miras (Gromadzki et al 2009), the S-type yellow symbiotic AE Cir (Mennickent et al 2008), and even in some single C-rich Miras like R Vol (Whitelock et al 1997). All of these share with M 2-29 similar depths and durations of fading events due to dust.…”

Section: Similarities With Yellow Symbiotic Starsmentioning

confidence: 99%

“…The Raman feature is therefore a sufficient but not necessary condition for a symbiotic star classification. Furthermore, even if M 2-29 had a primary hot enough to excite O VI, the curious appearance of the Raman lines in AE Cir only during obscuration (Mennickent et al 2008) means we might not expect to see them at all during light maximum when our VLT FLAMES spectra were taken. Another interesting example is CI Cygni which never shows the Raman lines and only episodically shows [Fe VII] lines (Mikołajewska & Ivison 2001).…”

Section: Similarities With Yellow Symbiotic Starsmentioning

confidence: 99%

“…Perhaps least understood are those variables that exhibit fading events due to dust obscuration. These include R Coronae Borealis stars (RCB, Clayton 1996), Population-I WC9 stars (Veen et al 1998;Kato et al 2002), symbiotic stars (Mikołajewska et al 1999;Mennickent et al 2008;Gromadzki et al 2009), PNe (Méndez et al 1982;Cohen et al 2002;Hajduk et al 2008, hereafter HZG08) stars with long secondary periods or LSPs (Wood et al 1999(Wood et al , 2004Soszyński 2007;Nicholls et al 2009;). …”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

The influence of binarity on dust obscuration events in the planetary nebula M 2-29 and its analogues

Miszalski¹,

Mikołajewska²,

Köppen³

et al. 2011

A&A

View full text Add to dashboard Cite

The central star of the planetary nebula (CSPN) M 2-29 shows an extraordinary R Coronae Borealis-like fading event in its optical lightcurve. The only other CSPN to show these events are CPD-56 • 8032 (Hen 3-1333) and V651 Mon (NGC 2346). Dust cloud formation in the line of sight appears responsible but the exact triggering mechanism is not well understood. Understanding how planetary nebulae (PNe) trigger dust obscuration events may help understand the same process in a wide range of objects including Population-I WC9 stars, symbiotic stars and perhaps asymptotic giant branch (AGB) stars with long secondary periods (LSPs). A binary scenario involving an eccentric, wide companion that triggers dust formation via interaction at periastron is a potential explanation that has been suggested for LSP variables. Model fits to the lightcurves of CPD-56 • 8032 and M 2-29 show the dust forms in excess of 70 AU at the inner edge of a dust disk. In the case of CPD-56 • 8032 this radius is far too large to coincide with a binary companion trigger, although a binary may have been responsible for the formation of the dust disk. We find no direct evidence to support previous claims of binarity in M 2-29 either from the OGLE lightcurve or deep medium-resolution VLT FLAMES spectroscopy of the CSPN. We classify the CSPN as Of(H) with T eff = 50 ± 10 kK and log g = 4.0 ± 0.3. We find a mean distance of 7.4 ± 1.8 kpc to M 2-29 at which the M V = −0.9 mag CSPN could potentially hide a subgiant luminosity or fainter companion. A companion would help explain the multiple similarities with D -type symbiotic stars whose outer nebulae are thought to be bona-fide PNe. The 7.4 kpc distance, oxygen abundance of 8.3 dex and Galactic coordinates ( = 4.0, b = −3.0) prove that M 2-29 is a Galactic Bulge PN and not a Halo PN as commonly misconceived.

show abstract

“…Then another study was conducted on V3885 Sgr (Ribeiro & Diaz 2007). This phenomenon was also detected on the symbiotic star candidate AE Cir (Mennickent et al 2008).…”

Section: Introductionmentioning

confidence: 54%

A Time-Series Analysis of the H$\alpha$ Emission Line in V3885 Sagitarii

Ribeiro

Diaz

2009

Publications of the Astronomical Society of Japan

View full text Add to dashboard Cite

Flickering is a phenomenon related to the mass accretion observed among many classes of astrophysical objects. In this paper we present a study of the flickering emission lines and continuum of the Cataclysmic Variable V3885 Sgr. The flickering behavior is first analyzed through statistical analysis and lightcurves power spectra. Autocorrelation techniques are then employed to estimate the flickering flares timescales. A cross correlation study between the line and its underlying continuum variability is presented. The cross correlation between the photometric and spectroscopic data is also discussed. The periodograms, calculated using emission line data, show a behavior that is similar to those obtained from photometric datasets found in the literature, with a plateau at lower frequencies and a power law at higher frequencies.The power law index is consistent with stochastic events. The cross-correlation study indicates the presence of a correlation between the variability on Hα and its underlying continuum. Flickering timescales derived from the photometric data were estimated as 25 minutes for two lightcurves and 10 minutes for one of them. The average timescales of the line flickering is 40 minutes, while for its underlying continuum it drops to 20 minutes.

show abstract

The remarkable properties of the symbiotic star AE Circinus

Cited by 5 publications

References 38 publications

Evidence for a [WR] or WEL-type binary nucleus in the bipolar planetary nebula Vy 1-2

Evidence for a [WR] or WEL-type binary nucleus in the bipolar planetary nebula Vy 1-2

The influence of binarity on dust obscuration events in the planetary nebula M 2-29 and its analogues

A Time-Series Analysis of the H$\alpha$ Emission Line in V3885 Sagitarii

Contact Info

Product

Resources

About